Show simple item record

dc.contributor.authorOjha, Roopesh
dc.contributor.authorLien, A.
dc.contributor.authorLee, W. H.
dc.contributor.authoret al.
dc.date.accessioned2020-03-10T16:59:33Z
dc.date.available2020-03-10T16:59:33Z
dc.date.issued2017-10-16
dc.description.abstractOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg² at a luminosity distance of 40₋₈⁺⁸ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the OneMeter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.en_US
dc.description.sponsorshipSee the paper for sponsorship too extension to reproduce here.en_US
dc.description.urihttps://iopscience.iop.org/article/10.3847/2041-8213/aa91c9en_US
dc.format.extent59 pagesen_US
dc.genrejournal articlesen_US
dc.identifierdoi:10.13016/m2dmyl-ejkq
dc.identifier.citationOjha, Roopesh; Kuin, N. P. M.; Eatough, R. P.; Multi-messenger Observations of a Binary Neutron Star Merger; The Astrophysical Journal Letters, Volume 848, Number 2 (2017); https://iopscience.iop.org/article/10.3847/2041-8213/aa91c9en_US
dc.identifier.urihttps://doi.org/10.3847/2041-8213/aa91c9
dc.identifier.urihttp://hdl.handle.net/11603/17526
dc.language.isoen_USen_US
dc.publisherThe American Astronomical Societyen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.relation.ispartofUMBC Joint Center for Earth Systems Technology (JCET)
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rightsThis work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law
dc.titleMulti-messenger Observations of a Binary Neutron Star Mergeren_US
dc.typeTexten_US


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record